Uranus and Neptune Models

The following tables contain the latest Uranus and Neptune models provided by the different authors below expressed in different units:

  • Uranus, Lellouch,, (see plots and explanatory note)
  • Uranus, Abbas, (see plots)
  • Uranus, Griffin & Orton, (see plots)

  • Neptune, Lellouch, (see plots and explanatory note)
  • Neptune, Abbas, (see plots and explanatory note) Note that the flux densities are given per unit solid angle. The planet's angular diameters at different dates can be found in the Astronomical Almanac. Typical values are 3".55 (==> 2.33E-10 sr) for Uranus, and 2".22 (==> 0.912E-10 sr) for Neptune.

    Model comparisons

    The differences in the fluxes predicted by the different models are typically smaller than 15%. Find here a comparison between the different Uranus models above.


    Important note:

    Currently, the LWS Relative Spectral Response Function (RSRF) is based on the Uranus model provided by Griffin & Orton while the absolute flux calibration of ISOPHT at long wavelengths is based on a combination of stars, asteroids and planets. For the planets, the Uranus and Neptune models provided by Abbas are used.

    The selection of the Griffin and Orton's model to derive the RSRF of LWS is supported by the good agreement found between this model and observations of Mars and other solar system objects at short wavelengths

    Last update: 28-07-2000 by Pedro Garcia-Lario